TY - JOUR
T1 - MERLIN polarimetry of the OH masers in IRAS 20406+2953
AU - Bains, I.
AU - Richards, A.M.S.
AU - Gledhill, T.
AU - Yates, J.A.
N1 - ‘The definitive version is available at www.blackwell-synergy.com '. Copyright Blackwell Publishing. [Full text of this article is not available in the UHRA]
PY - 2004
Y1 - 2004
N2 - We present the third in a series of results from our programme of the detection and measurement of magnetic fields in protoplanetary nebulae (PPN), using full-polarization MERLIN observations of OH masers. These are the first maps of the OH 1612- and 1667-MHz masing emission from IRAS 20406+2953. We have identified a Zeeman pair in the 1612-MHz data; this result heralds the second magnetic field strength measured in a PPN. We show that the field, of strength −3.1 mG, is sufficiently strong to be shaping the outflowing mass from the star. By considering the spatial distribution of the masers and the structure of the linear polarization data, we suggest a field configuration that is toroidal. The observed change in polarization position angle between the peak red- and blueshifted components of the maser features, if attributed to Faraday rotation within the circumstellar envelope, gives an electron density of ∼1 cm−3. We show that this is sufficient to freeze the field into the outflowing wind.
AB - We present the third in a series of results from our programme of the detection and measurement of magnetic fields in protoplanetary nebulae (PPN), using full-polarization MERLIN observations of OH masers. These are the first maps of the OH 1612- and 1667-MHz masing emission from IRAS 20406+2953. We have identified a Zeeman pair in the 1612-MHz data; this result heralds the second magnetic field strength measured in a PPN. We show that the field, of strength −3.1 mG, is sufficiently strong to be shaping the outflowing mass from the star. By considering the spatial distribution of the masers and the structure of the linear polarization data, we suggest a field configuration that is toroidal. The observed change in polarization position angle between the peak red- and blueshifted components of the maser features, if attributed to Faraday rotation within the circumstellar envelope, gives an electron density of ∼1 cm−3. We show that this is sufficient to freeze the field into the outflowing wind.
U2 - 10.1111/j.1365-2966.2004.08209.x
DO - 10.1111/j.1365-2966.2004.08209.x
M3 - Article
SN - 0035-8711
VL - 354
SP - 529
EP - 542
JO - Monthly Notices of the Royal Astronomical Society (MNRAS)
JF - Monthly Notices of the Royal Astronomical Society (MNRAS)
IS - 2
ER -